Magnetosphere Model

Tsyganenko T96 magnetic field driven by the real-time solar wind, last 24 hours · inputs provided by NOAA and WDC Kyoto

← Real-time measurements Satellite tracker

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Noon–midnight meridianGSM X–Z, Sun to the left

Closed field lineOpen (leaves the magnetopause) Tail lobe (beyond X = −30 Rₑ)Magnetopause (Shue et al. 1998)

Field lines traced from footpoints at 100 km altitude, magnetic latitude 50–80° every 2.5°, at noon (MLT 12) and midnight (MLT 0), projected on the GSM X–Z plane. The short line through the Earth is the dipole axis (tilt toward or away from the Sun).

Equatorial planeSM X–Y, seen from the north, Sun to the left

Equatorial crossing of field lines from footpoints at 60°, 63°, 66°, 69°, 72° 6.6 Rₑ (geostationary distance)Magnetopause

Colour: change of the field strength by the magnetospheric currents, |B(T96 + IGRF)| − |B(IGRF)|. Positive on the dayside (compression by the magnetopause currents), negative on the nightside (ring and tail currents). The closed curves show where field lines from fixed footpoint latitudes cross the equator: pushed in on the dayside, stretched out on the nightside.

Model inputs and resultsup to the selected time

Solar-wind dynamic pressure P_dyn (nPa)

Dst (nT)

IMF B_y and B_z, GSM (nT)

Magnetopause stand-off distance (Rₑ); dotted: 6.6 Rₑ

|B| at 6.6 Rₑ on the magnetic equator, noon and midnight (nT)

Dipole tilt (°, positive toward the Sun)

Each point is one model run. Drivers: 15-min means of the solar wind propagated to Earth (rows taken at their arrival time) and the last hourly Dst. Grey bands mark the T96 validity range; values outside it were clipped for the model run. Hover a plot to move the selected time.